Kinematic differences between multiple populations in Galactic globular clusters

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Volume 671 (March 2023)

A&A, 671 (2023) A106

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Table A.3.

Median and upper limits of the parameter distributions for the parametric model of each cluster.

Cluster	Population	v_max [km/s]	θ₀ [rad]	(v/σ)_HL	λ_R, HL	log₁₀(T_rh/yr)
NGC 104	Overall					9.55
	P1					–
	P2					–

NGC 362	Overall	< 1.0	–	< 0.03	< 0.028	8.93
	P1	< 5	–	< 0.09	< 0.07	–
	P2	< 4	–	< 0.07	< 0.06	–
	P3	< 15	–	< 0.4	< 0.3	–

NGC 1851	Overall					8.82
	P1					–
	P2					–
	P3					–

NGC 1904	Overall					8.95

NGC 2808	Overall					9.15
	P1					–
	P2					–

NGC 3201	Overall					9.27
	P1	< 10	–	< 0.3	< 0.24	–
	P2	< 9	–	< 0.3	< 0.23	–

NGC 5286	Overall					9.11
	P1					–
	P2					–
	P3					–

NGC 5904	Overall					9.41
	P1					–
	P2					–

NGC 6093	Overall					8.8
	P1					–
	P2					–

NGC 6218	Overall					8.87
	P1	< 9	–	< 0.29	< 0.23	–
	P2	< 6	–	< 0.25	< 0.20	–

NGC 6254	Overall					8.9
	P1	< 8	–	< 0.20	< 0.16	–
	P2	< 7	–	< 0.20	< 0.15	–

NGC 6266	Overall					8.98

NGC 6293	Overall					8.94

NGC 6388	Overall					8.9
	P1	< 20	–	< 0.17	< 0.12	–
	P2					–
	P3	< 11	–	< 0.15	< 0.12	–

NGC 6397	Overall	< 0.7	–	< 0.024	< 0.019	8.6
	P1	< 12	–	< 0.4	< 0.27	–
	P2	< 11	–	< 0.3	< 0.23	–

NGC 6441	Overall					9.09
	P1	< 9	–	< 0.05	< 0.04	–
	P2	< 5	–	< 0.029	< 0.022	–
NGC 6522	Overall	< 7	–	< 0.029	< 0.021	8.86

NGC 6541	Overall					9.03
	P1					–
	P2					–

NGC 6624	Overall					8.71
	P1	< 9	–	< 0.12	< 0.09	–
	P2	< 7	–	< 0.10	< 0.07	–

NGC 6656	Overall					9.23
	P1	< 8	–	< 0.5	< 0.3	–
	P2	< 7	–	< 0.4	< 0.28	–
	P3	< 7	–	< 0.4	< 0.3	–

NGC 6681	Overall	< 2.2	–	< 0.04	< 0.028	8.65
	P1	< 12	–	< 0.20	< 0.14	–
	P2	< 7	–	< 0.10	< 0.07	–

NGC 6752	Overall					8.87
	P1	< 12	–	< 0.18	< 0.13	–
	P2	< 9	–	< 0.12	< 0.09	–

NGC 7078	Overall					9.32
	P1	< 2.2	–	< 0.07	< 0.06	–
	P2					–

NGC 7089	Overall					9.4
	P1					–
	P2					–
	P3	< 11	–	< 0.4	< 0.3	–

NGC 7099	Overall					8.88
	P1	< 4	–	< 0.16	< 0.12	–
	P2	< 4	–	< 0.11	< 0.08	–

Notes. The two measures of the rotation strength (v/σ)_HL and λ_R, HL were derived from the parameter distribution of the parametric model, as described in Sect. 3.2. The median relaxation times T_rh for each cluster are from Harris (1996, 2010 edition).

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